Extending Anisotropic Interiors admitting Vanishing Complexity in Charged f (R, T) Theory

Abstract

This paper extends the definition of the complexity factor for a charged self‐gravitating structure in the background of gravity. For this purpose, the modified Einstein‐Maxwell field equations and the mass function in terms of interior charge are calculated corresponding to a static sphere. The Reissner‐Nordström exterior spacetime and match it with the spherical interior at the hypersurface to determine the junction conditions are adopted then. The curvature tensor is also decomposed orthogonally, resulting in several scalar functions. Only encompasses all the required parameters and fulfills the proposed criteria to be the complexity factor for the considered setup is noticed. Moreover, some constraints to minimize the degrees of freedom in the field equations are chosen. To achieve this, complexity‐free constraint with four additional conditions depending on the matter sector that lead to different models is employed. The stability of the developed models is also analyzed in the presence and absence of charge through the standard model by varying the values of the model parameter . The presence of charge in compact models corresponding to , a polytropic and a linear equation of state make them stable for specific values of is concluded.

Anisotropic extensions of isotropic Finch–Skea metric in the charged modified gravity

“…In this regard, junction conditions play a vital role in comprehending the overall structure of the geometrical system. The interior geometry is described by equation (28), and for the exterior region, we need a suitable metric. The selection of the latter geometry depends on the requirement that its basic properties must be compatible with the inner spacetime, such as the presence/absence of charge, static/nonstatic nature, etc.…”

“…The results indicate that the calculated masses of the considered pulsars aligned closely with the existing values. Furthermore, numerous studies focusing on stellar interiors within this theory have yielded promising and insightful outcomes [21][22][23][24][25][26][27][28][29].…”

Analysis of some newly constructed compact models in f(R, T) theory

“…This particular model has been adopted by Das et al [15] to construct a gravastar-like configuration comprising three distinct layers, each characterized by unique equations of state. Various methodologies have been employed to explore multiple stellar systems within the framework of this modified model from which remarkable results were obtained [16][17][18][19][20][21][22][23][24][25][26].…”